Evaluating (and Improving) Estimates of the Solar Radial Magnetic Field Component from Line-of-Sight Magnetograms

Abstract

Although for many solar physics problems the desirable or meaningful boundary is the radial component of the magnetic field $B_{\mathrm {r}}$ , the most readily available measurement is the component of the magnetic field along the line of sight to the observer, $B_{\mathrm {los}}$ . As this component is only equal to the radial component where the viewing angle is exactly zero, some approximation is required to estimate $B_{\mathrm {r}}$ at all other observed locations. In this study, a common approximation known as the “ $\mu$ -correction”, which assumes all photospheric field to be radial, is compared to a method that invokes computing a potential field that matches the observed $B_{\mathrm {los}}$ , from which the potential field radial component, $B_{\mathrm {r}}^{\mathrm {pot}}$ is recovered. We demonstrate that in regions that are truly dominated by a radially oriented field at the resolution of the data employed, the $\mu$ -correction performs acceptably if not better than the potential-field approach. However, it is also shown that for any solar structure that includes horizontal fields, i.e. active regions, the potential-field method better recovers both the strength of the radial field and the location of magnetic neutral line.